12-20 July 2017
BEXCO
Asia/Seoul timezone
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Contribution

BEXCO

[GA273] TAIGA - a hybrid detector complex for high energy gamma-ray astro-physics and cosmic ray physics in the Tunka valley

Speakers

  • Nikolay BUDNEV

Primary authors

Co-authors

  • R. WISCHNEWSKI (DESY, Germany)
  • A. ZAGORODNIKOV (Institute of Applied Physics ISU, Russia)
  • D. ZHUROV (Institute of Applied Physics ISU, Russia)
  • V. ZURBANOV (Institute of Applied Physics ISU, Russia)
  • I. YASHIN (National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russia)
  • M. TLUCZYKONT (Institut fur Experimentalphysik, University of Hamburg, Germany)
  • B. TARASHANSKY (Institute of Applied Physics ISU, Russia)
  • L. TKACHEV (JINR, Russia)
  • A. TKACHENKO (JINR, Russia)
  • L. SVESHNIKOVA (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • V. TABOLENKO (Institute of Applied Physics ISU, Russia)
  • V. SLUNECKA (JINR, Russia)
  • A. SOKOLOV (Novosibirsk State University, NSU, Russia)
  • A. SKURIKHIN (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • C. SPIERING (DESY, Germany)
  • A. SILAEV JR. (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • A. SIDORENKOV (Institute for Nuclear Research of RAN, Russia)
  • A. SILAEV (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • Yu SEMENEY (Institute of Applied Physics ISU, Russia)
  • V. SAMOLIGA (Institute of Applied Physics ISU, Russia)
  • B. SABIROV (JINR, Russia)
  • Y. SAGAN (JINR, Russia)
  • A. PUSHNIN (Institute of Applied Physics ISU, Russia)
  • G. RUBTSOV (Institute for Nuclear Research of RAN, Russia)
  • V. PTUSKIN (IZMIRAN, Russia)
  • E. RJABOV (Institute of Applied Physics ISU, Russia)
  • A. PORELLI (DESY, Germany)
  • E. POSTNIKOV (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • V. PROSIN (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • E. POPOVA (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • V. POLESCHUK (Institute of Applied Physics ISU, Russia)
  • M. POPESKU (ISS, Romania)
  • A. PETRUKHIN (National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russia)
  • L. PANKOV (Institute of Applied Physics ISU, Russia)
  • M. PANASYUK (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • E. OSIPOVA (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • A. PAKHORUKOV (Institute of Applied Physics ISU, Russia)
  • R. MONKHOEV (Institute of Applied Physics ISU, Russia)
  • R. NACHTIGALL (Institut fur Experimentalphysik, University of Hamburg, Germany)
  • Razmik MIRZOYAN (Max-Planck-Institute for Physics, Germany)
  • N. LUBSANDORZHIEV (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • R. MIRGAZOV (Institute of Applied Physics ISU, Russia)
  • B. LUBSANDORZHIEV (Institute for Nuclear Research of RAN, Russia)
  • V. LENOK (Institute of Applied Physics ISU, Russia)
  • Leonid KUZMICHEV (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • Yu LEMESHEV (Institute of Applied Physics ISU, Russia)
  • M. KUNNAS (Institut fur Experimentalphysik, University of Hamburg, Germany)
  • V. KOZHIN (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • E. KRAVCHENKO (Novosibirsk State University, NSU, Russia)
  • E. KOROSTELEVA (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • K. KOMPANIETS (National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russia)
  • S. KIRYUHIN (Institute of Applied Physics ISU, Russia)
  • R. KOKOULIN (National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russia)
  • V. KINDIN (National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russia)
  • A. IVANOVA (Institute of Applied Physics ISU, Russia)
  • Y. KAZARINA (Institute of Applied Physics ISU, Russia)
  • V. GREBENYUK (JINR, Russia)
  • A. GRINYUK (JINR, Russia)
  • N. KALMYKOV (Skobeltsyn Institute of Nuclear Physics MSU, Russia)
  • A. DYACHOK (Institute of Applied Physics ISU, Russia)
  • O. FEDOROV (Institute of Applied Physics ISU, Russia)
  • O. GRISHIN (Institute of Applied Physics ISU, Russia)
  • T. GRESS (Institute of Applied Physics ISU, Russia)
  • Oleg GRESS (Institute of Applied Physics ISU, Russia)
  • A. GAFAROV (Institute of Applied Physics ISU, Russia)
  • A. BORODIN (JINR, Russia)
  • M. BRUECKNER (DESY, Germany)
  • A. CHIAVASSA (Dipartimento di Fisica Generale Universiteta di Torino and INFN, Italy)
  • P. BEZYAZEEKOV (Institute of Applied Physics ISU, Russia)
  • I. ASTAPOV (National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Russia)

Description

The physics motivations and advantages of the new TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) detector are presented. TAIGA aims to addresses gamma-ray astronomy at energies from a few TeV to several PeV, as well as cosmic ray physics from 100 TeV to several EeV. For the energy range 30 – 200 TeV the sensitivity of 5 km^2 area TAIGA detector for the detection of local sources is expected to be 10^{−13} erg cm^{−2} sec^{−1} for 500 h of observations. Combination of the wide angle Cherenkov timing detector TAIGA-HiSCORE with the 4-m class Imaging Atmospheric Cherenkov Telescopes (TAIGA-IACT) of FoV of 10x10 degrees offers a cost effective-way to construct a 5 km^2 array. Reconstruction of a given EAS energy, incoming direction and its core position, based on the TAIGA-HiSCORE data allow one to increase a distance between the IACTs up to 1000-1200 m. The low investments together with the high sensitivity for energies ≥ 30-50 TeV make this pioneering technique very attractive for exploring the galactic PeVatrons and cosmic rays. In addition to the Cherenkov light detectors we intend to deploy an array of muon detectors (TAIGA-Muon array) spread over an area of 1 km^2 with a total area of about 2000 m^2. The TAIGA-IACT together with the TAIGA-Muon array will be used for selection of gamma-ray induced EAS. At present the TAIGA first stage has been constructed in Tunka valley, ~50 km West from the Lake Baikal. Now it consists of 28 TAIGA-HiSCORE Cherenkov stations distributed over an area of 0.25 km^2 and the first IACT of the TAIGA-IACT array. We are planning to test operation of the single telescope in coincidence with the HiSCORE up to shower impact distances of ~500-600 m; for this purpose we already started construction of the second imaging telescope on 300m distance from the first one. During 2017-2019 we intend to increase number of the TAIGA-HiSCORE stations up to 100-120 spread on the area of 1 km^2 and to deploy 1 - 2 additional IACTs of the TAIGA-IACT array. The first experimental results with the TAIGA first stage will be reported.